The macro-scale AGN feedback deposition channels are difficult to disentangle through simple temperature or surface brightness maps. The metal tracers are instead able to unveil in a clear manner such feedback features. Indeed, while the BGG produces a continuous reservoir of metals/iron in the core of the galaxy group, the self-regulated AGN outflows uplift them (Eq. REF ) outwards, on top of the low-\(Z\)  background, thus creating key contrast patterns and imprints.
Fig. REF  exemplifies this during a typical HR HD simulation [1]} of AGN feedback – self-regulated via CCA - in a galaxy group akin to NGC 5044 (with a central BGG \(M_\ast \simeq 3.4\times 10^{11}\,M_{\odot }\) ).
In the right panel, the meso AGN outflows have just uplifted the iron generated in the core of the BGG (magenta) up to several tens kpc. The pattern is highly anisotropic and the enhancement can reach up to \(\sim 2\times \)  values compared with the pristine background (\(<0.3\,Z_\odot \) , e.g. [2]}). Inhomogeneities are also visible, particularly the thin metal-rich rim that envelopes the inflated buoyant bubble.
At variance, in the left panel, as the AGN outflows subside and CCA feeding is quenched via the previous AGN outburst, the cascading subsonic turbulence drives mixing, eventually washing out the inhomogeneities (cavity, cocoon, jet channel) and restoring the azimuthally symmetric IGrM halo `weather'. Subsequently, this enables another phase of gradual IGrM precipitation and hence boosted accretion, with the triggering of another AGN feedback cycle via the condensed material.
Both the above-shown anisotropic metal outflows and turbulent distributions have been found by a wide range of hot halo observations involving mechanical AGN feedback (§REF ) and a diverse range of HD numerical studies and groups [3]}, [4]}, [5]}, [6]}, [7]}, [8]}, [9]}. We note that galactic SN-driven outflows, albeit weaker and difficult to spatially detect, can enhance the anisotropic enrichment, especially in low-mass halos [10]}, [11]}.
